In our spectral analysis, we can estimate the inner radius of the accretion disk (R\(_{in}\) ) in two different ways. The relxilllpCp model directly provides R\(_{in}\) , which is found to be 14.78\(^{+10.69}_{-14.78}\)  (r\(_{g}\) ) and 12.88\(^{+8.50}_{-3.74}\)  (r\(_{g}\) ), for epoch E1 and E2, respectively. R\(_{in}\)  can be calculated from the normalization of the diskbb model. Using the disc inclination obtained from our spectral analysis, taking the mass to be 4.9 M\(_\odot \)  [1]} and the distance to be 2.4 kpc [2]}, R\(_{in}\)  corresponding to epoch E1 and E2 found to be 0.66\(^{+0.13}_{-0.13}\)  (r\(_{g}\) ) and 1.12\(^{+0.12}_{-0.13}\)  (r\(_{g}\) ), respectively. We find that the R\(_{in}\)  values calculated from the normalization of the diskbb model are smaller than the values estimated from the relxilllpCp model. One possible reason for the discrepancy in the R\(_{in}\)  values is that the relxilllpCp model is not self-consistent as it uses the nthComp model with seed photon temperature (T\(_{bb}\) ) fixed at 0.05 keV. This value of T\(_{bb}\)  is uncharacteristically low for a stellar mass black hole accretion disk. As a result, a higher temperature component becomes necessary to represent a part of the existing cold disk. Secondly, [3]} carried out a critical analysis of the usual interpretation of the multicolor disc model parameters for black hole candidates in terms of the inner radius and temperature of the accretion disc. The authors have reported that the diskbb model underestimates the inner disk radius. [3]} suggested that when the disk contribution is very low and the spectrum is mostly dominated by non-thermal photons, the radius inferred by diskbb is inaccurate. They have also explained that it is very difficult to determine the exact shape of the accretion disk spectrum for the aforementioned case. [5]} suggested a correction factor to improve the value of R\(_{in}\)  calculated from diskbb.
